For stars with Teff \(>\)  8000 K, \(\log g\)  was derived by comparing the observed widths of the Balmer lines H\(\delta \) , H\(\gamma \)  and H\(\beta \)  at intensity 0.80 with those from the models ([1]}). The initial grid was interpolated in order to obtain the \(\log g\)  values that provide the best fit for each line, the final value being the average of the previous. Uncertainties were calculated from the standard deviation of the individual \(\log g\)  values obtained in each of the considered Balmer lines. Lines affected by strong emission components that do not allow to correctly trace the wings of the absorption profiles were excluded from the analysis (see an example in the top right panel of Fig. 2).
